| 1. | Work out how old the oldest chondrules are , and you know when the sun ignited
得出最老的陨石球粒的年龄，你就可以知道太阳是什么时候开始燃烧的。 |
| 2. | That chondrules formed in such quantities suggests that the heating which created them was widespread
这么大量的陨石球粒的形成说明能使它们形成的热量的范围很大。 |
| 3. | Looking at these isotopes allows the chondrules to be dated , and they were formed 4 . 56 billion years ago
观察这些同位素可以估算出陨石球粒的年龄，他们是在45 . 6亿年前形成的。 |
| 4. | To reach back , you need to look in the dust grains in chondrites , rather than at the chondrules
如果是追溯太阳系形成之前，你需要研究球粒状陨石中的灰尘颗粒，而不是陨石球粒。 |
| 5. | Like the chondrules themselves , most dust grains were created in the early solar system ? in this case by bigger objects grinding against each other
和陨石球粒他们一样，大部分灰尘创造于太阳系初期? ?这样的话，它们是较大物体相互摩擦产生的。 |
| 6. | Although such hypothetical chondrules should have been preserved , researchers have not yet found any . ( to be fair , though , scientists have only just begun to look
这种假设性的球粒应该能保存下来，但是研究人员至今仍尚未寻获（不过，公平说来，科学家也才刚开始寻找而已） 。 |
| 7. | Because the chondritic asteroids formed after the chondrules did , the initial 26al to 27al ratio in chondrules places an upper limit on the amount of 26al that was available to heat the rocky bodies
因为球粒陨石小行星是在球粒之后形成，球粒中铝26对铝27的初始比值，决定了能够用来加热石质天体的铝26含量的上限。 |
| 8. | According to this scenario , researchers could never find evidence of such early chondrules because all these objects would have been destroyed by the melting of the chondritic asteroids into which they accreted
在这个情形下，研究人员恐怕永远也无法找到如此早期的球粒证据，因为所有这些物体在聚合的过程中，都会因为球粒陨石小行星熔化而被破坏。 |
| 9. | These investigations have found strong evidence for the former presence of 26al in the so - called refractory inclusions : tiny mineral assemblages , rich in calcium and aluminum , embedded in chondritic meteorites alongside the chondrules
这些研究发现了强而有力的证据，显示铝26曾经存在于所谓的耐火包体（富含钙和铝的细小矿物组合体，与球粒一起镶埋在球粒陨石内） 。 |
| 10. | Given the decay rate of 26al , the lower initial ratio in the chondrules implies that these objects formed between one million and two million years after the creation of the refractory inclusions ( assuming that the radioisotope was indeed homogeneously distributed in the early solar system )
以铝26的衰变速率估计，这些球粒的初始比值较低，表示它们是在耐火包体产生后100 ~ 200万年才形成（假设铝26在早期太阳系中确实是均匀分布的） 。 |
